  We present optical, ultraviolet, and infrared data of the type II supernova
(SN II) 2020jfo at 14.5 Mpc. This wealth of multiwavelength data allows to
compare different metrics commonly used to estimate progenitor masses of SN II
for the same object. Using its early light curve, we infer SN 2020jfo had a
progenitor radius of $\approx$700 $R_{\odot}$, consistent with red supergiants
of initial mass $M_{\rm ZAMS}=$11-13 $M_{\odot}$. The decline in its late-time
light curve is best fit by a ${}^{56}$Ni mass of 0.018$\pm$0.007 $M_{\odot}$
consistent with that ejected from SN II-P with $\approx$13 $M_{\odot}$ initial
mass stars. Early spectra and photometry do not exhibit signs of interaction
with circumstellar matter, implying that SN 2020jfo experienced weak mass loss
within the final years prior to explosion. Our spectra at $>$250 days are best
fit by models from 12 $M_{\odot}$ initial mass stars. We analyzed integral
field unit spectroscopy of the stellar population near SN 2020jfo, finding its
massive star population had a zero age main sequence mass of
9.7$\substack{+2.5\\-1.3} M_{\odot}$. We identify a single counterpart in
pre-explosion imaging and find it has an initial mass of at most
$7.2\substack{+1.2\\-0.6} M_{\odot}$. We conclude that the inconsistency
between this mass and indirect mass indicators from SN 2020jfo itself is most
likely caused by extinction with $A_{V}=2$-3 mag due to matter around the
progenitor star, which lowered its observed optical luminosity. As SN 2020jfo
did not exhibit extinction at this level or evidence for interaction with
circumstellar matter between 1.6-450 days from explosion, we conclude that this
material was likely confined within $\approx$3000 $R_{\odot}$ from the
progenitor star.
