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We present late-time images of the site of the peculiar jet-driven TypeIIn supernova SN2010jp, including HST images taken 2-5 yr post explosion and deep ground-based images over a similar time. These are used to characterise its unusually remote environment and to constrain the progenitor's initial mass and age. The position of SN2010jp is found to reside along a chain of diffuse starlight that is probably an outer spiral arm or tidal tail of the interacting galaxy pair NGC2207/IC2163. There is one bright HII region projected within 1 kpc, and there is faint extended Halpha emission immediately surrounding the continuum source at the position of SN2010jp, which has $M_{F555W} = -7.7 (\pm 0.2)$ mag. In principle, the lingering light could arise from late-time circumstellar material (CSM) interaction, an evolved supergiant, a host star cluster, or some combination of these. Steady flux over 3 yr and a lack of strong, spatially unresolved Halpha emission make ongoing CSM interaction unlikely. If an evolved supergiant dominates, its observed luminosity implies an initial mass of roughly 22 $M_{\odot}$ and an age older than roughly 8 Myr. If the source is a star cluster, then its colour and absolute magnitude imply an age of 8-13 Myr and a modest cluster initial mass of log($M/M_{\odot}$) = 3.6-3.8. Extended Halpha emission out to a radius of 30 pc reveals a faint evolved HII region, pointing to recent star formation with at least one late O-type star. Based on these various clues, we conclude that the progenitor of SN2010jp had a likely initial mass of 18-22 $M_{\odot}$.