  I present results of the analysis of a set of images obtained in the field of
the Milky Way globular cluster NGC 6362 using the Dark Energy Camera, which is
mounted in the 4.0m Victor Blanco telescope of the Cerro-Tololo Interamerican
observatory. The cluster was selected as a science case for deep high-quality
photometry because of the controversial observational findings and theoretical
predictions on the existence of cluster tidal tails. The collected data allowed
us to build an unprecedented deep cluster field color-magnitude diagram, from
which I filtered stars to produce a stellar density map, to trace the stellar
density variation as a function of the position angle for different concentric
annulii centered on the cluster, and to construct a cluster stellar density
radial profile. I also built a stellar density map from a synthetic
color-magnitude diagram generated from a model of the stellar population
distribution in the Milky Way. All the analysis approached converge toward a
relatively smooth stellar density between 1 and $\sim$ 3.8 cluster Jacobi
radii, with a slightly difference smaller than 2 times the background stellar
density fluctuation between the mean stellar density of the south-eastern and
that of north-western hemispheres, the latter being higher. Moreover, the
spatial distribution of the recently claimed tidal tail stars agrees well not
only with the observed composite star field distribution, but also with the
region least affected by interstellar absorption. Nevertheless, I detected a
low stellar density excess around the cluster Jacobi radius, from which I
conclude that NGC 6362 present a thin extra tidal halo.
