We report on the properties of the low-mass stars that recently formed in the central \sim 2 \farcm 7 \times 2 \farcm 7 of 30 Dor including the R 136 cluster .
Using the photometric catalogue of De Marchi et al .
( 2011c ) , based on observations with the Hubble Space Telescope ( HST ) , and the most recent extinction law for this field , we identify 1 035 bona-fide pre-main sequence ( PMS ) stars showing H \alpha excess emission at the 4 \sigma level with H \alpha equivalent width of 20 Å or more .
We find a wide spread in age spanning the range \sim 0.1 - 50 Myr .
We also find that the older PMS objects are placed in front of the R 136 cluster and are separated from it by a conspicuous amount of absorbing material , indicating that star formation has proceeded from the periphery into the interior of the region .
We derive physical parameters for all PMS stars , including masses m , ages t , and mass accretion rates \dot { M } _ { acc } .
To identify reliable correlations between these parameters , which are intertwined , we use a multivariate linear regression fit of the type \log \dot { M } _ { acc } = a \times \log t + b \times \log m + c .
The values of a and b for 30 Dor are compatible with those found in NGC 346 and NGC 602 .
We extend the fit to a uniform sample of 1 307 PMS stars with 0.5 < m /M { { } _ { \odot } } < 1.5 and t < 16 Myr in six star forming regions in the Large and Small Magellanic Clouds and Milky Way with metallicities in the range 0.1 - 1.0 Z _ { \odot } .
We find a = -0.59 \pm 0.02 and b = 0.78 \pm 0.08 .
The residuals are systematically different between the six regions and reveal a strong correlation with metallicity Z , of the type c = ( -3.69 \pm 0.02 ) - ( 0.30 \pm 0.04 ) \times \log Z / Z _ { \odot } .
A possible interpretation of this trend is that when the metallicity is higher so is the radiation pressure and this limits the accretion process , both in its rate and duration .