(U)LIRGs form stars 10-100 times more efficiently than main sequence (MS) galaxies, which is explained by nearby (U)LIRGs being gas-rich merging galaxies. Numerical simulations and sub- kpc observations clearly show that tidal interaction between gas-rich progenitors is condensing gas and triggering subsequent starburst activity in the nuclear region and throughout the extended disk. However, it remains unclear if the properties of their GMCs, as the sites for star formation, themselves differ as well from those in normally star-forming galaxies. The bvious difference would potentially imply important changes to current theories. Before ALMA it was impossible to study GMCs in (U)LIRGs. This poster presents short-spacing corrected 40-120 pc resolution CO(2-1) data for seven nearby (U)LIRGs, and compare basic statistical GMC properties between nearby (U)LIRGs and nearby main sequence galaxies from the PHANGS- ALMA large program.