We present a comprehensive analysis of four young open clusters, NGC 663, NGC 2301, NGC 2384, and NGC 7510, utilizing high-precision astrometric and photometric data from Gaia DR3. Cluster membership was determined using the UPMASK algorithm, resulting in probable member counts ranging from 337 to 1498 across the clusters. Bayesian Markov Chain Monte Carlo isochrone fitting yielded cluster ages in the range 7.0–8.15, with uncertainties of ∼0.11–0.18. Reddening values ranged from E(B − V) = 0.093 mag in NGC 2301 to 1.24 mag in NGC 7510, consistent with their positions near the Galactic plane. The stellar mass function slopes (α ≈ 2.00–2.26) closely match the Salpeter IMF, with total stellar masses spanning nearly an order of magnitude, from ∼486 M⊙ in NGC 2301 to ∼3584 M⊙ in NGC 663. Dynamical relaxation times indicate that only NGC 2301 (τ ≈ 10.00) and NGC 2384b (τ ≈ 2.03) are dynamically relaxed; the others remain dynamically evolving. Orbital integrations in the MWPotential2014 model reveal nearly circular Galactic orbits with very low eccentricities (e ≈ 0.003–0.014) and small vertical distances ( kpc), confirming their confinement to the thin disk. SED and kinematic analyses show that NGC 2384a & b are separated by ∼0.55 kpc, indicating an optical pair.

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