The phenomenon of multiple stellar populations (MPs), characterised by star-to-star variations in light-element abundances, is a ubiquitous feature of globular clusters (GCs). While spectroscopic surveys have directly revealed these abundance anomalies, photometric studies, particularly with the Hubble Space Telescope (HST), have been instrumental in characterizing MP sequences across the colour-magnitude diagrams (CMDs). However, the narrow field of view of the HST has restricted these studies to only a small portion of the star clusters, leaving the vast majority of the clusters’ space unexplored. The upcoming Chinese Space Station Survey Telescope (CSST), with its wide field of view and both UV and optical capabilities, will provide new opportunities for systematic MP studies. We aim to quantify the capability of the CSST wide-field camera in detecting and characterizing MPs in GCs through virtual simulations that closely mimic real observations. We performed comprehensive simulations using synthetic stellar population models incorporating different helium abundances (ΔY) and carbon-nitrogen-oxygen (CNO) variations. We simulated CSST observations for GCs at distances of about 9.6 kpc and 20 kpc with different exposure times. We evaluated the detection efficiency of MPs based on the CMDs constructed from the seven different bands of the CSST, as well as the pseudo color–color diagrams (chromosome diagrams) designed with the UV-optical combination. For a GC at a distance of approximately 9.6 kpc, the NUV − u color index of the CSST is highly sensitive to stellar populations with different ΔY and CNO abundances in the CMD, providing color separations of Δ(NUV − u) ≈ 0.16 (for red giants) to 0.44 mag (for dwarfs). We find that when the total exposure time in the UV band exceeds ∼1000 s and the exposure time in the optical band exceeds ∼300 s, the main survey camera of CSST is sufficient to resolve these MPs. Furthermore, extending the simulations to 20 kpc, a distance encompassing ∼80% of Galactic GCs, we demonstrate that the SCam retains significant diagnostic power, resolving stellar populations with ΔY ≥ 0.06 dex and δ[N/Fe] ≥ 0.64 dex, and distinguishing MPs in the CMD down to i ∼ 19.5 mag for clusters with substantial chemical dispersions. The combination of NUV–u–g filters provides diagnostic capabilities comparable to HST’s F275W–F336W–F438W system. CSST will be a powerful facility for MP studies, capable of efficiently surveying the entire spatial extent of several hundred star clusters in the local group. Its wide field of view and multi-band capabilities will enable the first homogeneous MP census spanning the entire Milky Way and its neighbouring galaxies, significantly advancing our understanding of star clusters’ formation and chemical evolution.