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The iMaNGA project uses a forward-modelling approach to compare thepredictions of cosmological simulations with observations from SDSS-IV/MaNGA.We investigate the dependency of age and metallicity radial gradients on galaxymorphology, stellar mass, stellar surface mass density ($\Sigma_*$), andenvironment. The key of our analysis is that observational biases affecting theinterpretation of MaNGA data are emulated in the theoretical iMaNGA sample. Thesimulations reproduce the observed global stellar population scaling relationswith positive correlations between galaxy mass and age/metallicity quite welland also produce younger stellar populations in late-type in agreement withobservations. We do find interesting discrepancies, though, that can inform thephysics and further development of the simulations. Ages of spiral galaxies andlow-mass ellipticals are overestimated by about 2-4 Gyr. Radial metallicitygradients are steeper in iMaNGA than in MaNGA, a discrepancy most prominent inspiral and lenticular galaxies. Also, the observed steepening of metallicitygradients with increasing galaxy mass is not well matched by the simulations.We find that the theoretical radial profiles of surface mass density $\Sigma_*$are steeper than in observations except for the most massive galaxies. In bothMaNGA and iMaNGA [Z/H] correlates with $\Sigma_*$, however, the simulationssystematically predict lower [Z/H] by almost a factor of 2 at any $\Sigma_*$.Most interestingly, for galaxies with stellar mass $\log M_*\leq 10.80 M_\odot$the MaNGA data reveal a positive correlation between galaxy radius and [Z/H] atfixed $\Sigma_*$, which is not recovered in iMaNGA. Finally, the dependence onenvironmental density is negligible in both the theoretical iMaNGA and theobserved MaNGA data.

iMaNGA: mock MaNGA galaxies based on IllustrisTNG and MaStar SSPs. -- III. Stellar metallicity drivers in MaNGA and TNG50