  Kilonovae are ultraviolet, optical, and infrared transients powered by the
radioactive decay of heavy elements following a neutron star merger. Joint
observations of kilonovae and gravitational waves can offer key constraints on
the source of Galactic $r$-process enrichment, among other astrophysical
topics. However, robust constraints on heavy element production requires rapid
kilonova detection (within $\sim 1$ day of merger) as well as multi-wavelength
observations across multiple epochs. In this study, we quantify the ability of
13 wide field-of-view instruments to detect kilonovae, leveraging a large grid
of over 900 radiative transfer simulations with 54 viewing angles per
simulation. We consider both current and upcoming instruments, collectively
spanning the full kilonova spectrum. The Roman Space Telescope has the highest
redshift reach of any instrument in the study, observing kilonovae out to $z
\sim 1$ within the first day post-merger. We demonstrate that BlackGEM, DECam,
GOTO, the Vera C. Rubin Observatory's LSST, ULTRASAT, and VISTA can observe
some kilonovae out to $z \sim 0.1$ ($\sim$475 Mpc), while DDOTI, MeerLICHT,
PRIME, $Swift$/UVOT, and ZTF are confined to more nearby observations.
Furthermore, we provide a framework to infer kilonova ejecta properties
following non-detections and explore variation in detectability with these
ejecta parameters.
