  We present an analysis of spatially resolved gas-phase metallicity relations
in five dwarf galaxies ($M_{halo} \approx 10^{11} M_\odot$, $M_\star \approx
10^{8.8}-10^{9.6} M_\odot$) from the FIRE-2 (Feedback in Realistic
Environments) cosmological zoom-in simulation suite, which include an explicit
model for sub-grid turbulent mixing of metals in gas, near $z\approx 0$, over a
period of 1.4 Gyrs, and compare our findings with observations. While these
dwarf galaxies represent a diverse sample, we find that all simulated galaxies
match the observed mass-metallicity (MZR) and mass-metallicity gradient (MZGR)
relations. We note that in all five galaxies, the metallicities are effectively
identical between phases of the interstellar medium (ISM), with 95$\%$ being
within $\pm$0.1 dex between various ISM phases, including the cold and dense
gas ($T < 500$ K and $n_{\rm H} > 1$ cm$^{-3}$), ionized gas (near the
H$\alpha$ $T \approx 10^4$ K ridge-line), and nebular regions (ionized gas
where the 10 Myr-averaged star formation rate is non-zero). We find that most
of the scatter in relative metallicity between cold and dense gas and ionized
gas/nebular regions can be attributed to either local starburst events or
metal-poor inflows. We also note the presence of a major merger in one of our
galaxies, m11e, with a substantial impact on the metallicity distribution in
the spatially resolved map, showing two strong metallicity peaks and triggering
a starburst in the main galaxy.
