  We present optical imaging and spectroscopy of SN\,2018lfe, which we classify
as a Type I superluminous supernova (SLSN-I) at a redshift of $z = 0.3501$ with
a peak absolute magnitude of $M_r\approx -22.1$ mag, one of the brightest SLSNe
discovered. SN\,2018lfe was identified for follow-up using our FLEET machine
learning pipeline. Both the light curve and the spectra of SN\,2018lfe are
consistent with the broad population of SLSNe. We fit the light curve with a
magnetar central engine model and find an ejecta mass of $M_{\rm ej}\approx
3.8$ M$_\odot$, a magnetar spin period of $P\approx 2.9$ ms and a magnetic
field strength of $B_{\perp}\approx 2.8\times 10^{14}$ G. The magnetic field
strength is near the top of the distribution for SLSNe, while the spin period
and ejecta mass are near the median values of the distribution for SLSNe. From
late-time imaging and spectroscopy we find that the host galaxy of SN\,2018lfe
has 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 formation
rate of $\approx 0.8$ M$_\odot$ yr$^{-1}$.
