  (Abridged) Sulfur chemistry is poorly understood in the process of low-mass
star and planet formation, where the main carriers of sulfur are still unknown.
Despite the fact that simple S-bearing molecules are usually detected toward
embedded sources, large surveys of S-bearing molecules with high angular
resolution and sensitive observations are currently lacking. The goal of this
work is to present an unbiased survey of simple sulfur-bearing species in
protostars and provide new statistics. In addition, we investigate the role of
S-bearing molecules in accretion processes and the connection between
(non-)detection of complex organic molecules (COMs) and S-related species. We
present the observations of sulfur-bearing species that are part of the Perseus
ALMA Chemical Survey (PEACHES). We analyzed a total of 50 Class 0/I sources
with an average angular resolution of about 0.6" (~180 au) in ALMA band 6. We
present detection rates for CS, SO, 34SO, and SO2. The SO/34SO ratio is lower
than the canonical value of 22 and the lowest values are found for those
sources rich in COMs. This ratio, therefore, seems to be a good tracer of the
inner high-density envelope. The detection of multiple COMs seems to be related
to the presence of collimated outflows and SO2 emission seems to trace the warm
gas in those sources where CH3OH is also detected. The SO2 abundances toward
the PEACHES sample are, on average, two orders of magnitude lower than values
from the Ophiuchus star-forming region and comparable with sources in Taurus,
suggesting that the sulfur depletion in the gas-phase could depend on the
external UV radiation. Finally, the SO2 emission detected in different
evolutionary stages seems to arise from different physical mechanisms: high
column density of warm material in Class 0 sources, shocks in Class I/II, and
exposure to UV radiation from the protostar in more evolved Class II disks.
