The outer disk of the Large Magellanic Cloud (LMC) is studied in order to unveil clues about its formation and evolution. We have obtained deep color-magnitude diagrams and low resolution spectroscopy for red giant stars in six fields with galactocentric distances from 5.2 kpc to 9.2 kpc and different azimuths. The color-magnitude diagrams shows that while the oldest population is approximately coeval in all fields, the age of the youngest populations increases with increasing radius. Radial velocities and stellar metallicities have been obtained from low-resolution spectra in the infrared Ca II triplet region. The metal content of the most metal-poor objects, which are also the oldest according to the derived age-metallicity relationships, is similar in all fields independently of the galactocentric distance. However, while the metallicity of the most metal-rich objects measured, which are the youngest ones, remains constant in the inner 6 kpc, it decreases with increasing radius from there on. According to the derived age-metallicity relationships, which are consistent with being the same in all fields, this result may be interpreted as an outside-in formation scheme in opposition with the inside-out scenario predicted by ΛCDM cosmology for a galaxy like the LMC. The analysis of the radial velocities of our sample of giants shows that they follow a rotational cold disk kinematics. The velocity dispersion increases as metallicity decreases indicating that the most metal-poor/oldest objects are distributed in a thicker disk than the most metal-rich/youngest ones in agreement with the findings in other disks such as that of the Milky Way. They do not seem to be part of a hot halo, if one exists in the LMC.