Stellar chemical abundances encode the formation and evolutionary history of the Galactic disc. The bimodality observed in the plane has been widely interpreted as evidence of distinct thin- and thick-disc populations. We analysed the chemical, spatial, and kinematic properties of stars in the solar neighbourhood using the Dark Energy Spectroscopic Instrument (DESI) Data Release 1 combined with astrometry, aiming to characterize the low-α and high-α populations and their evolutionary connections. Gaia We constructed a high-quality sample of FGK dwarf stars by applying rigorous selection criteria to stellar parameters, abundances, and distances. We employed Gaussian mixture modelling to statistically separate low-α and high-α stars and examined their metallicity distribution functions (MDFs), vertical and radial gradients, and kinematics. The DESI solar neighbourhood sample reveals a clear bimodality. The low-α stars dominate near the Galactic mid-plane, with a broad MDF peaking at and negative vertical and radial metallicity gradients of mathrm d Fe/H / |Z| ∼ -0.06 dex kpc d -1 d Fe / H ∼ -0.5^ d -1 ), an approximately flat radial profile of metallicity, and dynamically hotter kinematics. Nevertheless, the Toomre diagram shows substantial overlap between these chemically defined populations in velocity space, indicating that chemical abundance does not uniquely map to distinct kinematic components. These results indicate that the low-α and high-α populations underwent distinct chemical enrichment histories despite their substantial overlap in present-day kinematics. The observed chemo-dynamical properties point to the combined effects of chemical enrichment, radial redistribution, and secular dynamical evolution, underscoring the necessity of integrating stellar chemistry with kinematics to constrain the evolution of the Galactic disc.