To reveal the initial condition of star formation, we conducted numerical simulations of the formation and evolution of molecular clouds incorporating simplified chemical reactions, thermal processes, and self-gravity. We found that the global physical properties of molecular clouds are determined mainly by the angle at which the atomic gas is compressed relative to the magnetic field. Turbulence-dominated molecular clouds form when the atomic gas is accumulated almost along the magnetic field. As the angle increases, the magnetic energy becomes dominant over the turbulent energy (Iwasaki et al. 2019). Unlike the global properties of molecular clouds, the dense clumps, which are the site of star formation, are found to have universal properties (Iwasaki & Tomida 2022).