  In this work, we report the discovery of a candidate planetary-mass object
with a photoevaporating protoplanetary disk, Proplyd 133-353, which is near the
massive star $\theta^{1}$ Ori C at the center of the Orion Nebula Cluster
(ONC). The object was known to have extended emission pointing away from
$\theta^{1}$ Ori C, indicating ongoing external photoevaporation. Our
near-infrared spectroscopic data suggests that the central source of Proplyd
133-353 is substellar ($\sim$M9.5), might have a mass probably less than 13
Jupiter mass and an age younger than 0.5 Myr. Proplyd 133-353 shows a similar
ratio of X-ray luminosity to stellar luminosity to other young stars in the ONC
with a similar stellar luminosity, and has a similar proper motion to the mean
one of confirmed ONC members. We propose that Proplyd 133-353 was formed in a
very low-mass dusty cloud near $\theta^{1}$ Ori C as a second-generation of
star formation, which can explain both its young age and the presence of its
disk.
