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In this study we present the results of a five-year follow-up campaign of thelong-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host ofnear-solar metallicity. The long rise time (57 $\pm$ 2 days, ATLAS $o$ band)and high luminosity (peaking at $-$20.78 $\pm$ 0.01 mag in the ATLAS $o$ band)point towards an interaction of massive ejecta with massive and densecircumstellar material (CSM). The evolution of SN 2017hcc is slow, bothspectroscopically and photometrically, reminiscent of the long-lived type IIn,SN 2010jl. An infrared (IR) excess was apparent soon after the peak, andblueshifts were noticeable in the Balmer lines starting from a few hundreddays, but appeared to be fading by around +1200 days. We posit that an IR lightecho from pre-existing dust dominates at early times, with some possiblecondensation of new dust grains occurring at epochs >$\sim$+800 days.

A long life of excess: The interacting transient SN 2017hcc