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We present the results from a multi-year radio campaign of the superluminoussupernova (SLSN) 2017ens, which yielded the earliest radio detection of a SLSNto date at the age of $\sim$3.3 years after explosion. SN2017ens was notdetected at radio frequencies in the first $\sim$300\,d of evolution butreached $L_{\nu}\approx 10^{28}\,\rm{erg\,s^{-1}\,cm^{-2}}$ at $\nu\sim 6$ GHz,$\sim1250$ days post-explosion. Interpreting the radio observations in thecontext of synchrotron radiation from the supernova shock interaction with thecircumstellar medium (CSM), we infer an effective mass-loss rate of $\approx10^{-4}\,\rm{M_{\odot}yr^{-1}}$ at $r\sim 10^{17}$ cm from the explosion'ssite, for a wind speed of $v_w=50-60\,\rm{km\,s^{-1}}$ measured from opticalspectra. These findings are consistent with the spectroscopic metamorphosis ofSN2017ens from hydrogen-poor to hydrogen-rich $\sim190$ d after explosionreported by Chen et al., 2018. SN2017ens is thus an addition to the sample ofhydrogen-poor massive progenitors that explode shortly after having lost theirhydrogen envelope. The inferred circumstellar densities, implying a CSM mass upto $\sim0.5\,\rm{M_{\odot}}$, and low velocity of the ejection point at binaryinteractions (in the form of common envelope evolution and subsequent envelopeejection) playing a role in shaping the evolution of the stellar progenitors ofSLSNe in the $\lesssim 500$ yr preceding core collapse.

Luminous Radio Emission from the Superluminous Supernova 2017ens at 3.3 years after explosion