  Ultraviolet (UV) galaxies have been selected from GALEX. The presence of a
FUV-dropout in their spectral energy distributions proved to be a very complete
(83.3%) but not very efficient (21.4%) tool for identifying Lyman Break
Galaxies (LBGs) at z~1. We divide the LBG sample into two sub-classes: red LBGs
(RLBGs) detected at 24 micron which are mainly Luminous IR Galaxies (LIRGs) and
blue LBGs (BLBGs) undetected at 24 microns down to 83 microJy. Two of the RLBGs
are also detected at 70 micron. The median SED of the RLBGs is similar (above
lambda~1 micron) to the dusty starburst HR10. However, unlike local (U)LIRGs,
RLBGs are UV bright objects. We suggest that these objects contain a large
amount of dust but that some bare stellar populations are also directly
visible. The median SED of the BLBGs is consistent with their containing the
same stellar population as the RLBGs but with a lower dust content. The
luminosity function of our LBG sample at z~1 is similar to the luminosity
function of NUV-selected galaxies at the same redshift. The integrated
luminosity densities of z~1 LBGs and NUV-selected galaxies are very consistent.
We show that star formation rates (SFRs) estimated from UV measurements and
corrected using the IRX-beta method provide average total SFR_TOT in agreement
with SFR_UV + SFR_dust. However, IRX-beta-based SFR_TOT shows a large
dispersion. Summing up the detected UV (1150A rest-frame) and IR-based star
formation rates of the detected objects, we find that only one third of the
total (i.e. UV + dust) LBG SFR resides in BLBGs and two thirds in RLBGs, even
though most LBGs at z~1 are BLBGs. On the other hand, the total SFR of LBGs
accounts for only 11% of the total SFR at z~1. Finally, we observe a regular
decrease of L_TIR / L_FUV from z=0 to z~2 for UV-selected samples.
