Based on the high-resolution 12CO, 13CO and C18O J = 1 − 0 observations from the Purple Mountain Observatory 13.7 m millimeter telescope, atomic hydrogen (H i) spectral data from the Five-hundred-meter Aperture Spherical radio Telescope, and Herschel far-infrared data, we present a multi-wavelength study toward a giant molecular filament, GMF54.0-52.0 (hereafter G53). We investigated the transition from the cold H i gas, which is associated with the molecular gas of G53, to molecular hydrogen (H2) gas based on the H i narrow self-absorption (HINSA) feature. The mean/median abundance of HINSA is 3.6/1.4 × 10−3, comparable to that of nearby low-mass star-forming molecular clouds. The abundances present low values in the dense region inside G53 and higher values surrounding it, revealing that the atomic-to-molecular transition is more complete in G53. We derived a chemical age of ∼2.6 ± 0.04 to ∼4.5 ± 0.1 Myr for the filament, which is comparable to previous studies on the ages of interstellar clouds and clumps. G53 is located at the interaction boundary between two expanding H i bubbles. The dynamical ages of the two bubbles are ∼6.2–11.7 Myr and ∼6.6–9.1 Myr, respectively, longer than the chemical age of G53. We suggest that the G53 molecular filament originated from the compression of the cold H i gas at the shared boundary of these bubbles.