  We perform a systematic study of evolutionary stages and stellar masses of
young stellar objects (YSOs) in the Large Magellanic Cloud (LMC) to investigate
properties of star formation of the galaxy. There are 4825 sources in our YSO
sample, which are constructed by combining the previous studies identifying
YSOs in the LMC. Spectral energy distributions of the YSOs from optical to
infrared wavelengths were fitted with a model consisting of stellar, polycyclic
aromatic hydrocarbon and dust emissions. We utilize the stellar-to-dust
luminosity ratios thus derived to study the evolutionary stages of the sources;
younger YSOs are expected to show lower stellar-to-dust luminosity ratios. We
find that most of the YSOs are associated with the interstellar gas across the
galaxy, which are younger with more gases, suggesting that more recent star
formation is associated with larger amounts of the interstellar medium (ISM).
N157 shows a hint of higher stellar-to-dust luminosity ratios between active
star-forming regions in the LMC, suggesting that recent star formation in N157
is possibly in later evolutionary stages. We also find that the stellar mass
function tends to be bottom-heavy in supergiant shells (SGSs), indicating that
gas compression by SGSs may be ineffective in compressing the ISM enough to
trigger massive star formation. There is no significant difference in the
stellar mass function between YSOs likely associated with the interface between
colliding SGSs and those with a single SGS, suggesting that gas compression by
collisions between SGSs may also be ineffective for massive star formation.
