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Star formation is a hierarchical process, forming young stellar structures ofstar clusters, associations, and complexes over a wide scale range. Thestar-forming complex in the bar region of the Large Magellanic Cloud isinvestigated with upper main-sequence stars observed by the VISTA Survey of theMagellanic Clouds. The upper main-sequence stars exhibit highly non-uniformdistributions. Young stellar structures inside the complex are identified fromthe stellar density map as density enhancements of different significancelevels. We find that these structures are hierarchically organized such thatlarger, lower-density structures contain one or several smaller, higher-densityones. They follow power-law size and mass distributions as well as a lognormalsurface density distribution. All these results support a scenario ofhierarchical star formation regulated by turbulence. The temporal evolution ofyoung stellar structures is explored by using subsamples of upper main-sequencestars with different magnitude and age ranges. While the youngest subsample,with a median age of log($\tau$/yr)~=~7.2, contains most substructure,progressively older ones are less and less substructured. The oldest subsample,with a median age of log($\tau$/yr)~=~8.0, is almost indistinguishable from auniform distribution on spatial scales of 30--300~pc, suggesting that the youngstellar structures are completely dispersed on a timescale of $\sim$100~Myr.These results are consistent with the characteristics of the 30~Doradus complexand the entire Large Magellanic Cloud, suggesting no significant environmentaleffects. We further point out that the fractal dimension may bemethod-dependent for stellar samples with significant age spreads.

The VMC Survey XXVII. Young Stellar Structures in the LMC$'$s Bar Star-Forming Complex