  We investigate the nature of an unusually faint member of the $\epsilon$ Cha
Association ($D\sim100$ pc, age $\sim5$ Myr), the nearest region of star
formation of age $<$8 Myr. This object, 2MASS J11550336-7919147 (2M1155$-$79B),
is a wide ($\sim$580 AU) separation, comoving companion to low-mass (M3)
$\epsilon$ Cha Association member 2MASS J11550485-7919108 (2M1155$-$79A). We
present near-infrared spectra of both components, along with analysis of
photometry from Gaia EDR3, 2MASS, VHS, and WISE. The near-IR spectrum of
2M1155$-$79B displays strong He I 1.083 emission, a sign of active accretion
and/or accretion-driven winds from a circumstellar disk. Analysis of WISE
archival data reveals that the mid-infrared excess previously associated with
2M1155$-$79A instead originates from the disk surrounding 2M1155$-$79B. Based
on these results, as well as radiative transfer modeling of its optical/IR
spectral energy distribution, we conclude that 2M1155$-$79B is most likely a
young, late-M, star that is partially obscured by, and actively accreting from,
a nearly edge-on circumstellar disk. This would place 2M1155$-$79B among the
rare group of nearby ($D\lesssim100$ pc), young (age $<$10 Myr) mid-M stars
that are orbited by and accreting from highly inclined protoplanetary disks.
Like these systems, the 2M1155$-$79B system is a particularly promising subject
for studies of star and planet formation around low-mass stars.

Solar and Stellar Astrophysics;Earth and Planetary Astrophysics