  We present the detection and analysis of molecular hydrogen emission toward
ten interstellar regions in the Large Magellanic Cloud. We examined
low-resolution infrared spectral maps of twelve regions obtained with the
Spitzer infrared spectrograph (IRS). The pure rotational 0--0 transitions of
H$_2$ at 28.2 and 17.1${\,\rm \mu m}$ are detected in the IRS spectra for ten
regions. The higher level transitions are mostly upper limit measurements
except for three regions, where a 3$\sigma$ detection threshold is achieved for
lines at 12.2 and 8.6${\,\rm \mu m}$. The excitation diagrams of the detected
H$_2$ transitions are used to determine the warm H$_2$ gas column density and
temperature. The single-temperature fits through the lower transition lines
give temperatures in the range $86-137\,{\rm K}$. The bulk of the excited H$_2$
gas is found at these temperatures and contributes $\sim$5-17% to the total gas
mass. We find a tight correlation of the H$_2$ surface brightness with
polycyclic aromatic hydrocarbon and total infrared emission, which is a clear
indication of photo-electric heating in photodissociation regions. We find the
excitation of H$_2$ by this process is equally efficient in both atomic and
molecular dominated regions. We also present the correlation of the warm H$_2$
physical conditions with dust properties. The warm H$_2$ mass fraction and
excitation temperature show positive correlations with the average starlight
intensity, again supporting H$_2$ excitation in photodissociation regions.
