  The Galactic Bulge can uniquely be studied from large samples of individual
stars, and is therefore of prime importance for understanding the stellar
population structure of bulges in general. Here the observational evidence on
the kinematics, chemical composition, and ages of Bulge stellar populations
based on photometric and spectroscopic data is reviewed. The bulk of Bulge
stars are old and span a metallicity range -1.5<~[Fe/H]<~+0.5. Stellar
populations and chemical properties suggest a star formation timescale below ~2
Gyr. The overall Bulge is barred and follows cylindrical rotation, and the more
metal-rich stars trace a Box/Peanut (B/P) structure. Dynamical models
demonstrate the different spatial and orbital distributions of metal-rich and
metal-poor stars. We discuss current Bulge formation scenarios based on
dynamical, chemical, chemodynamical and cosmological models. Despite impressive
progress we do not yet have a successful fully self-consistent chemodynamical
Bulge model in the cosmological framework, and we will also need more extensive
chrono-chemical-kinematic 3D map of stars to better constrain such models.
