  We present the JWST Resolved Stellar Populations Early Release Science (ERS)
science program. We obtained 27.5 hours of NIRCam and NIRISS imaging of three
targets in the Local Group (Milky Way globular cluster M92, ultra-faint dwarf
galaxy Draco II, star-forming dwarf galaxy WLM), which span factors of
$\sim10^5$ in luminosity, $\sim10^4$ in distance, and $\sim10^5$ in surface
brightness. We describe the survey strategy, scientific and technical goals,
implementation details, present select NIRCam color-magnitude diagrams (CMDs),
and validate the NIRCam exposure time calculator (ETC). Our CMDs are among the
deepest in existence for each class of target. They touch the theoretical
hydrogen burning limit in M92 ($<0.08$ $M_{\odot}$; SNR $\sim5$ at
$m_{F090W}\sim28.2$; $M_{F090W}\sim+13.6$), include the lowest-mass stars
observed outside the Milky Way in Draco II (0.09 $M_{\odot}$; SNR $=10$ at
$m_{F090W}\sim29$; $M_{F090W}\sim+12.1$), and reach $\sim1.5$ magnitudes below
the oldest main sequence turnoff in WLM (SNR $=10$ at $m_{F090W}\sim29.5$;
$M_{F090W}\sim+4.6$). The PARSEC stellar models provide a good qualitative
match to the NIRCam CMDs, though are $\sim0.05$ mag too blue compared to M92
F090W$-$F150W data. The NIRCam ETC (v2.0) matches the SNRs based on photon
noise from DOLPHOT stellar photometry in uncrowded fields, but the ETC may not
be accurate in more crowded fields, similar to what is known for HST. We
release beta versions of DOLPHOT NIRCam and NIRISS modules to the community.
Results from this ERS program will establish JWST as the premier instrument for
resolved stellar populations studies for decades to come.
