  We study the hierarchical stellar structures in a $\sim$1.5 deg$^2$ area
covering the 30 Doradus-N158-N159-N160 star-forming complex with the VISTA
Survey of the Magellanic Clouds. Based on the young upper main-sequence stars,
we find that the surface densities cover a wide range of values, from
log($\Sigma\cdot$pc$^2$) $\lesssim$ $-$2.0 to log($\Sigma\cdot$pc$^2$)
$\gtrsim$ 0.0. Their distributions are highly non-uniform, showing groups that
frequently have sub-groups inside. The sizes of the stellar groups do not
exhibit characteristic values, and range continuously from several parsecs to
more than 100 pc; the cumulative size distribution can be well described by a
single power law, with the power-law index indicating a projected fractal
dimension $D_2$ = 1.6 $\pm$ 0.3. We suggest that the phenomena revealed here
support a scenario of hierarchical star formation. Comparisons with other
star-forming regions and galaxies are also discussed.
