  Context. The measurement of $\alpha$-elements abundances provides a powerful
tool to put constraints on chemical evolution and star formation history of
galaxies. The majority of studies on the $\alpha$-element Sulfur (S) are
focused on local stars, making S behavior in other environments an astronomical
topic yet to be analyzed. Aims. The investigation of S in the Galactic bulge
has only recently been considered for the first time. This work aims to improve
our knowledge on S behavior in this component of the Milky Way. Methods. We
present S abundances of 74 dwarf and sub-giant stars in the Galactic bulge, 21
and 30 F and G thick and thin disk stars. We performed local thermodynamic
equilibrium analysis and applied corrections for non-LTE on high resolution and
high signal-to-noise UVES spectra. S abundances were derived from multiplets 1,
6 and 8 in the metallicity range $-2<$[Fe/H]$<$0.6, by spectrosynthesis or line
equivalent widths. Results. We confirm that S behaves like an $\alpha$-element
within the Galactic bulge. In the [S/Fe] versus [Fe/H] diagram, S presents a
plateau at low metallicity followed by a decreasing of [S/Fe] with the
increasing of [Fe/H], until reaching [S/Fe]$\sim0$ at super-solar metallicity.
We found that the Galactic bulge is S-rich with respect to both the thick and
thin disks at $-1<$[Fe/H]$<0.3$, supporting a more rapid formation and chemical
evolution of the Galactic bulge than the disk.
