Illustration showing a possible planet formation scenario. Here we envision a disk containing an MRI-inactive dead zone near the midplane (α_Dr(= α_Dz)∕α_acc ≪ 1), while the outer disk is active (α_Dr(= α_Dz)∕α_acc ~ 1). We also envision an initially high F_p/g value that becomes smaller with time, while the snow line moves inward. Our results of planetesimal formation around the snow line imply that the icy pebble pile-up (i.e., icy planetesimals formation by GI and/or SI; panel A) would be favored in the outer region (α_Dz ∕α_acc ~ 1) in the early stage of the evolution, while the formation of rocky planetesimals by GI of silicate dust would be favored in the later stage when the snow line has reached the dead zone (α_Dz ∕α_acc ≪ 1; panel C). In the intermediate phase (α_Dz∕α_acc < 1 but not α_Dz∕α_acc ≪ 1) and F_p/g < 0.6, SI/GI of pebbles and GI of silicate dust would not be expected to occur (panel B). A diversity of evolutionary paths for protoplanetary disks would produce a diversity of planetary systems.