Aims .
Filamentary structures of early type stars are found to be a common feature of the Magellanic Clouds formed at an age of about 0.9 - 2 \times 10 ^ { 8 } yr .
As we go to younger ages these large structures appear fragmented and sooner or later form young clusters and associations .
In the optical domain we have detected 56 such large structures of young objects , known as stellar complexes in the LMC for which we give coordinates and dimensions .
We also investigate star formation activity and evolution of these stellar complexes and define the term “ starburst region ” .
Methods .
IR properties of these regions have been investigated using IRAS data .
A colour-magnitude diagram ( CMD ) and a two-colour diagram from IRAS data of these regions ware compared with observations of starburst galaxies and cross-matching with HII regions and SNRs was made .
Radio emission maps at 8.6-GHz and the CO ( 1 \rightarrow 0 ) line were also cross correlated with the map of the stellar complexes .
Results .
It has been found that nearly 1/3 of the stellar complexes are extremely active resembling the IR behaviour of starburst galaxies and HII regions .
These stellar complexes illustrating such properties are called here “ starburst regions ” .
They host an increased number of HII regions and SNRs .
The main starburst tracers are their IR luminosity ( F _ { 60 } well above 5.4 Jy ) and the 8.6-GHz radio emission .
Finally the evolution of all stellar complexes is discussed based on the CO emission .