  We have discovered a young M star of mass $0.16\,M_\odot$ and radius
$0.63\,R_\odot$, likely in the Upper Sco Association, that exhibits only a
single $80\%$ deep occultation of 1-day duration. The star has frequent flares
and a low-amplitude rotational modulation, but is otherwise quiet over 160 days
of cumulative observation during K2 Campaigns C2 and C15. We discuss how such a
deep eclipse is not possible by one star crossing another in any binary or
higher-order stellar system in which no mass transfer has occurred. The two
possible explanations we are left with are (1) orbiting dust or small particles
(e.g., a disk bound to a smaller orbiting body, or unbound dust that emanates
from such a body); or (2) a transient accretion event of dusty material near
the corotation radius of the star. In either case, the time between such
occultation events must be longer than $\sim$80 days. We model a possible
orbiting occulter both as a uniform elliptically shaped surface (e.g., an
inclined circular disk) and as a `dust sheet' with a gradient of optical depth
behind its leading edge. The required masses in such dust features are then
$\gtrsim 3 \times 10^{19}$ g and $\gtrsim 10^{19}$ g, for the two cases,
respectively.
