We conducted observations of ^ { 12 } CO ( J = 5 - 4 ) and dust thermal continuum emission toward twenty star-forming galaxies on the main sequence at z \sim 1.4 using ALMA to investigate the properties of the interstellar medium . The sample galaxies are chosen to trace the distributions of star-forming galaxies in diagrams of stellar mass - star formation rate and stellar mass - metallicity . We detected CO emission lines from eleven galaxies . The molecular gas mass is derived by adopting a metallicity-dependent CO-to-H _ { 2 } conversion factor and assuming a CO ( 5-4 ) /CO ( 1-0 ) luminosity ratio of 0.23 . Molecular gas masses and its fractions ( molecular gas mass / ( molecular gas mass + stellar mass ) ) for the detected galaxies are in the ranges of ( 3.9 - 12 ) \times 10 ^ { 10 } ~ { } M _ { \odot } and 0.25 - 0.94 , respectively ; these values are significantly larger than those in local spiral galaxies . The molecular gas mass fraction decreases with increasing stellar mass ; the relation holds for four times lower stellar mass than that covered in previous studies , and that the molecular gas mass fraction decreases with increasing metallicity . Stacking analyses also show the same trends . The dust thermal emissions were clearly detected from two galaxies and marginally detected from five galaxies . Dust masses of the detected galaxies are ( 3.9 - 38 ) \times 10 ^ { 7 } ~ { } M _ { \odot } . We derived gas-to-dust ratios and found they are 3-4 times larger than those in local galaxies . The depletion times of molecular gas for the detected galaxies are ( 1.4 - 36 ) \times 10 ^ { 8 } ~ { } \mathrm { yr } while the results of the stacking analysis show \sim 3 \times 10 ^ { 8 } ~ { } \mathrm { yr } . The depletion time tends to decrease with increasing stellar mass and metallicity though the trend is not so significant , which contrasts with the trends in local galaxies .