  We surveyed nearly all the embedded protostars in seven nearby clouds (Corona
Australis, Aquila, Chamaeleon I & II, Ophiuchus North, Ophiuchus, Serpens) with
the Atacama Large Millimeter/submillimeter Array at 1.3mm observations with a
resolution of 0.1$"$. This survey detected 184 protostellar disks, 90 of which
were observed at a resolution of 14-18 au, making it one of the most
comprehensive high-resolution disk samples across various protostellar
evolutionary stages to date. Our key findings include the detection of new
annular substructures in two Class I and two flat-spectrum sources, while 21
embedded protostars exhibit distinct asymmetries or substructures in their
disks. We find that protostellar disks have a substantially large variability
in their radii across all evolutionary classes. In particular, the fraction of
large disks with sizes above 60\,au decreases as the protostar evolves from
Class 0 to Class I. Compiling the literature data, we discovered an increasing
trend of the gas disk radii to dust disk radii ratio ($R_{\rm gas,Kep}/R_{\rm
mm}$) with increasing bolometric temperature (${\rm T}_{\rm bol}$). Our results
indicate that the dust and gas disk radii decouple during the early Class I
stage. However, in the Class 0 stage, the dust and gas disk sizes are similar,
which allows a direct comparison between models and observational data at the
earliest stages of protostellar evolution. We show that the distribution of
radii in the 52 Class 0 disks in our sample is in high tension with various
disk formation models, indicating that protostellar disk formation remains an
unsolved question.
