  The putative host galaxy of FRB 20171020A was first identified as ESO
601-G036 in 2018, but as no repeat bursts have been detected, direct
confirmation of the host remains elusive. In light of recent developments in
the field, we re-examine this host and determine a new association confidence
level of 98%. At 37 Mpc, this makes ESO 601-G036 the third closest FRB host
galaxy to be identified to date and the closest to host an apparently
non-repeating FRB (with an estimated repetition rate limit of < 0.011 bursts
per day above 10 erg). Due to its close distance, we are able to perform
detailed multi-wavelength analysis on the ESO 601-G036 system. Follow-up
observations confirm ESO 601-G036 to be a typical star-forming galaxy with HI
and stellar masses of log(M_HI/M_sol) ~ 9.2 and log(M_*/M_sol) = 8.64, and a
star formation rate of SFR = 0.09 +/- 0.01 M_sol/yr. We detect, for the first
time, a diffuse gaseous tail (log(M_HI/M_sol) ~ 8.3) extending to the
south-west that suggests recent interactions, likely with the confirmed nearby
companion ESO 601-G037. ESO 601-G037 is a stellar shred located to the south of
ESO 601-G036 that has an arc-like morphology, is about an order of magnitude
less massive, and has a lower gas metallicity that is indicative of a younger
stellar population. The properties of the ESO 601-G036 system indicate an
ongoing minor merger event, which is affecting the overall gaseous component of
the system and the stars within ESO 601-G037. Such activity is consistent with
current FRB progenitor models involving magnetars and the signs of recent
interactions in other nearby FRB host galaxies.
