The 1.3mm CAMPOS survey has resolved 90 protostellar disks with ~15 au resolution across the Ophiuchus, Corona Australis, and Chamaeleon star-forming regions. To address the fundamental question, 'When does planet formation begins, we combined the CAMPOS sample with literature observations of Class 0-II disks (bolometric temperature, T_bol_<=1900K), all mapped at 1.3mm with resolutions ranging from 4 to 33au. To investigate substructure detection rates as a function of bolometric temperature, we restricted the sample to disks observed at the 1.3mm wavelength, with inclinations below 75 degrees, linear resolution <=20au and resolved with at least four resolution elements ({theta}_distk_/{theta}_res_?=4). We also considered the effects of extinction correction and the inclusion of Herschel Space Telescope data on the bolometric temperature measurements to constrain the lower and upper limits of bolometric temperature for each source. We find that by T_bol_~200-400K, substructure detection rates increased sharply to ~60%, corresponding to an approximate age of 0.2-0.4Myr. No substructures are detected in Class 0 disks. The ratio of disk-averaged brightness temperature to predicted dust temperature shows a trend of increasing values toward the youngest Class 0 disks, suggesting higher optical depths in these early stages. Our statistical analysis confirms that substructures similar to those in Class II disks are already common by the Class I stage, and the emergence of these structures at T_bol_~200-400K could represent only an upper limit. Classifying disks with substructures into those with and without large central cavities, we find both populations coexisting across evolutionary stages, suggesting they are not necessarily evolutionarily linked. If protostellar disk substructures do follow an evolutionary sequence, then our results imply that disk substructures evolve very rapidly and thus can be present in all Class I/II stages and/or that they can be triggered at different times.