  In recent years, our understanding of solar-like oscillations from main
sequence to red giant stars has improved dramatically thanks to pristine data
collected from space telescopes. One of the remaining open questions focuses
around the observational identification of solar-like oscillations in pre-main
sequence stars.
  We aim to develop an improved method to search for solar-like oscillations in
pre-main sequence stars and apply it to data collected by the Kepler K2
mission. Our software APOLLO includes a novel way to detect low signal-to-noise
ratio solar like oscillations in the presence of a high background level.
  By calibrating our method using known solar-like oscillators from the main
Kepler mission, we apply it to T Tauri stars observed by Kepler K2 and identify
several candidate pre-main sequence solar-like oscillators. We find that our
method is robust even when applied to time-series of observational lengths as
short as those obtained with the TESS satellite in one sector. We identify EPIC
205375290 as a possible candidate for solar-like oscillations in a pre-main
sequence star with $\nu_\mathrm{max} \simeq 242\,\mu$Hz. We also derive EPIC
205375290's fundamental parameters to be $T_\mathrm{eff}$ = 3670$\pm$180 K, log
$g$ = 3.85$\pm$0.3, $v$sin$i$ = 8 $\pm$ 1 km s$^{-1}$, and about solar
metallicity from a high-resolution spectrum obtained from the Keck archive.
