  The identification and localization of Fast Radio Bursts to their host
galaxies has revealed important details about the progenitors of these
mysterious, millisecond-long bursts of coherent radio emission. In this work we
study the most probable host galaxy of the apparently non-repeating CHIME/FRB
event FRB 20190425A -- a particularly high luminosity, low dispersion measure
event that was demonstrated by Moroianu et al. 2022 to be temporally and
spatially coincident with the LIGO-Virgo-KAGRA binary neutron star merger
GW190425, suggesting an astrophysical association (p-value 0.0052). In this
paper we remain agnostic to this result, and we confirm UGC10667 as the most
probable host galaxy of FRB 20190425A, demonstrating that the host galaxies of
low dispersion measure, one-off CHIME FRBs can be plausibly identified. We then
perform multi-wavelength observations to characterize the galaxy and search for
any afterglow emission associated with the FRB and its putative GW counterpart.
We find no radio or optical transient emission in our observations
$2.5\,\mathrm{yr}$ post-burst. UGC10667 is a spiral galaxy at $z\sim0.03$,
dominated by an old stellar population. We find no evidence of a large
population of young stars, with nebular emission dominated by star formation at
a rate of $1-2\,\mathrm{M_\odot\,yr^{-1}}$. While we cannot rule out a young
magnetar as the origin of FRB 20190425A, our observations are consistent with
an origin in a long delay-time neutron star binary merger as posited by
Moroianu et al. 2022.
