  We provide a homogeneous set of structural parameters of 83 star clusters
located at the periphery of the Small Magellanic Cloud (SMC) and the Large
Magellanic Cloud (LMC). The clusters' stellar density and surface brightness
profiles were built from deep, AO assisted optical images, and uniform analysis
techniques. The structural parameters were obtained from King and Elson et al.
model fittings. Integrated magnitudes and masses (for a subsample) are also
provided. The sample contains mostly low surface brightness clusters with
distances between 4.5 and 6.5 kpc and between 1 and 6.5 kpc from the LMC and
SMC centres, respectively. We analysed their spatial distribution and
structural properties, comparing them with those of inner clusters. Half-light
and Jacobi radii were estimated, allowing an evaluation of the Roche volume
tidal filling. We found that: (i) for our sample of LMC clusters, the tidal
radii are, on average, larger than those of inner clusters from previous
studies; (ii) the core radii dispersion tends to be greater for LMC clusters
located towards the southwest, with position angles of $\sim$200 degrees and
about $\sim$5 degrees from the LMC centre, i.e., those LMC clusters nearer to
the SMC; (iii) the core radius evolution for clusters with known age is similar
to that of inner clusters; (iv) SMC clusters with galactocentric distances
closer than 4 kpc are overfilling; (v) the recent Clouds collision did not
leave marks on the LMC clusters' structure that our analysis could reveal.
