  We present maps of the ionized gas flux distributions, excitation,
star-formation rate SFR, surface mass density $\Sigma_{H+}$, and obtain total
values of SFR and ionized gas masses {\it M} for 62 Active Galactic Nuclei
(AGN) observed with SDSS-IV MaNGA and compare them with those of a control
sample of 112 non-active galaxies. The most luminous AGN -- with
$L(\rm{[OIII]}\lambda 5007) \ge 3.8\times 10^{40}\,\mbox{erg}\,\mbox{s}^{-1}$,
and those hosted by earlier-type galaxies are dominated by Seyfert excitation
within 0.2 effective radius $R_e$ from the nucleus, surrounded by LINER
excitation or transition regions, while the less luminous and hosted by
later-type galaxies show equally frequent LINER and Seyfert excitation within
$0.2\,R_e$. The extent $R$ of the region ionized by the AGN follows the
relation $R\propto\,L(\rm{[OIII]})^{0.5}$ -- as in the case of the Broad-Line
Region. The SFR distribution over the region ionized by hot stars is similar
for AGN and controls, while the integrated SFR -- in the range
$10^{-3}-10$\,M$_\odot$\,yr$^{-1}$ is also similar for the late-type
sub-sample, but higher in the AGN for 75\% of the early-type sub-sample. We
thus conclude that there is no signature of AGN quenching star formation in the
body of the galaxy in our sample. We also find that 66\% of the AGN have higher
ionized gas masses $M$ than the controls -- in the range
10$^5-3\times10^7$\,M$_\odot$ -- while 75\% of the AGN have higher
$\Sigma_{H+}$ within $0.2\,R_e$ than the control galaxies.

Astrophysics of Galaxies