  In some planet formation theories, protoplanets grow gravitationally within a
young star's protoplanetary disk, a signature of which may be a localized
disturbance in the disk's radial and/or vertical structure. Using time-series
photometric observations by the Kilodegree Extremely Little Telescope South
(KELT-South) project and the All-Sky Automated Survey for SuperNovae (ASAS-SN),
combined with archival observations, we present the discovery of two extended
dimming events of the young star, DM Ori. This young system faded by $\sim$1.5
mag from 2000 March to 2002 August and then again in 2013 January until 2014
September (depth $\sim$1.7 mag). We constrain the duration of the 2000-2002
dimming to be $<$ 860 days, and the event in 2013-2014 to be $<$ 585 days,
separated by $\sim$12.5 years. A model of the spectral energy distribution
(SED) indicates a large infrared excess consistent with an extensive
circumstellar disk. Using basic kinematic arguments, we propose that DM Ori is
likely being periodically occulted by a feature (possibly a warp or
perturbation) in its circumstellar disk. In this scenario, the occulting
feature is located $>$6 AU from the host star, moving at $\sim$14.6 km/s, and
is $\sim$4.9 AU in width. This localized structure may indicate a disturbance
such as may be caused by a protoplanet early in its formation.
