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We present optical imaging and spectroscopy of SN\,2018lfe, which we classifyas a Type I superluminous supernova (SLSN-I) at a redshift of $z = 0.3501$ witha peak absolute magnitude of $M_r\approx -22.1$ mag, one of the brightest SLSNediscovered. SN\,2018lfe was identified for follow-up using our FLEET machinelearning pipeline. Both the light curve and the spectra of SN\,2018lfe areconsistent with the broad population of SLSNe. We fit the light curve with amagnetar central engine model and find an ejecta mass of $M_{\rm ej}\approx3.8$ M$_\odot$, a magnetar spin period of $P\approx 2.9$ ms and a magneticfield strength of $B_{\perp}\approx 2.8\times 10^{14}$ G. The magnetic fieldstrength is near the top of the distribution for SLSNe, while the spin periodand ejecta mass are near the median values of the distribution for SLSNe. Fromlate-time imaging and spectroscopy we find that the host galaxy of SN\,2018lfehas an absolute magnitude of $M_r\approx -17.85$, ($L_B \approx 0.029$ $L^*$),and an inferred metallicity of $Z\approx 0.3$ Z$_\odot$, and star formationrate of $\approx 0.8$ M$_\odot$ yr$^{-1}$.

Optical Observations and Modeling of the Superluminous Supernova 2018lfe