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Open clusters are one of the best astrophysical laboratories we have available for stellar astrophysics studies. This work presents metallicities and individual abundances for 14 M dwarfs and six G dwarfs from two well-known open clusters: Hyades and Coma Berenices. Our analysis is based on near-infrared (1.51–1.69μm), high-resolution (R∼ 22,500) spectra obtained from the Sloan Digital Sky Survey (SDSS) IV/APOGEE Survey. Using one-dimensional, plane-parallel MARCS model atmospheres, the APOGEE line list, and the Turbospectrum radiative transfer code in local thermodynamic equilibrium, we derived spectroscopic stellar parameters for the M dwarfs, along with abundances of 13 elements (C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe) for both M and G dwarfs. We find a high degree of chemical homogeneity within each cluster when comparing abundances derived from M and G dwarfs:δ[M/H] (M dwarfs–G dwarfs) of 0.01 ± 0.04, and 0.02 ± 0.03 for the Hyades and Coma Berenices, respectively. The overall cluster metallicities derived from M dwarfs (Hyades: 0.16 ± 0.03 and Coma Berenices: 0.02 ± 0.06) are consistent with previous literature determinations. Finally, we demonstrate the value of M dwarfs as key tracers in Galactic archeology, emphasizing their potential for studying Galactic metallicity gradients and chemical evolution.