  Chemical abundance variations in the ISM provide important information about
the galactic evolution, star-formation and enrichment histories. Recent
observations of disk galaxies suggest that if large-scale azimuthal metallicity
variations appear in the ISM, they are linked to the spiral arms. In this work,
using a set of chemodynamical simulations of the Milky Way-like spiral
galaxies, we quantify the impact of gas radial motions~(migration) in the
presence of a pre-existing radial metallicity gradient and the local ISM
enrichment on both global and local variations of the mean ISM metallicity in
the vicinity of the spiral arms.
  In all the models, we find the scatter of the gas metallicity of
\approx0.04-0.06 dex at a given galactocentric distance. On large scales, we
observe the presence of spiral-like metallicity patterns in the ISM which are
more prominent in models with the radial metallicity gradient. However, in our
simulations, the morphology of the large-scale ISM metallicity distributions
significantly differs from the spiral arms structure in stellar/gas components
resulting in both positive and negative residual~(after subtraction of the
radial gradient) metallicity trends along spiral arms. We discuss the
correlations of the residual ISM metallicity values with the star formation
rate, gas kinematics and offset to the spiral arms, concluding that the
presence of a radial metallicity gradient is essential for the azimuthal
variations of metallicity. At the same time, the local enrichment alone is
unlikely to drive systematic variations of the metallicity across the spirals.
