  We present a study of the internal structure of 82 star clusters located at
the outer regions of the Large Magellanic Cloud and the Small Magellanic Cloud
using data of the VISCACHA Survey. Through the construction of the minimum
spanning tree, which analyzes the relative position of stars within a given
cluster, it was possible to characterize the internal structure and explore the
fractal or subclustered distribution for each cluster. We computed the
parameters m (which is the average length of the connected segments normalized
by the area), s (which is the mean points separation in units of cluster
radius), and Q (the ratio of these components). These parameters are useful to
distinguish between radial, homogeneous, and substructured distributions of
stars. The dependence of these parameters with the different characteristics of
the clusters, such as their ages and spatial distribution, was also studied. We
found that most of the studied clusters present a homogeneous stellar
distribution or a distribution with a radial concentration. Our results are
consistent with the models, suggesting that more dynamically evolved clusters
seem to have larger Q values, confirming previous results from numerical
simulations. There also seems to be a correlation between the internal
structure of the clusters and their galactocentric distances, in the sense that
for both galaxies, the more distant clusters have larger Q values. We also paid
particular attention to the effects of contamination by non-member field stars
and its consequences finding that field star decontamination is crucial for
these kinds of studies.
