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Abstract This study provides a detailed examination of the structural, astrophysical, kinematic, and dynamical properties of the open clusters COIN-Gaia~24, Czernik~24, FSR~0893, and UBC~74, which are located in the opposite direction to the Galactic center. Astrometric, photometric, and spectroscopic data from the {\it Gaia} Data Release 3 catalog were used to ensure a precise characterization of cluster members and their physical properties. Membership determination was performed using the \texttt{UPMASK} algorithm applied to a five-dimensional parameter space, yielding 116, 179, 238, and 387 likely members for each cluster, respectively. Structural parameters were derived by fitting King profiles to the radial density distributions of high-probability members. Astrophysical parameters were estimated through Bayesian Markov chain Monte Carlo isochrone fitting based on \texttt{PARSEC} evolution models, complemented by spectral energy distribution analysis using \texttt{ARIADNE}. The resulting extinctions, distances, metallicities, and ages indicate that these are moderately reddened, intermediate-age clusters located between 1 and 3.5 kpc from the Sun. Mean radial velocities combined with Galactic orbital integrations computed with \texttt{galpy}, show that all four clusters follow nearly circular, low-eccentricity orbits typical of thin-disc populations. All four OCs have dynamical relaxation times of 22-98~Myr. Yet, their ages surpass these times by several factors, particularly in Czernik~24, revealing that they are dynamically evolved systems even though the calculated $T_{\rm E}$ values represent lower limits. The results confirm that these OCs serve as reliable tracers of the Galactic thin disc’s chemical and dynamical evolution.