  The next generation of space-based observatories will characterize the
atmospheres of low-mass, temperate exoplanets with the direct-imaging
technique. This will be a major step forward in our understanding of exoplanet
diversity and the prevalence of potentially habitable conditions beyond the
Earth. We compute a list of currently known exoplanets detectable with the
mid-infrared Large Interferometer For Exoplanets (LIFE) in thermal emission. We
also compute the list of known exoplanets accessible to a notional design of
the Habitable Worlds Observatory (HWO), observing in reflected starlight. With
a pre-existing method, we processed the NASA Exoplanet Archive and computed
orbital realizations for each known exoplanet. We derived their mass, radius,
equilibrium temperature, and planet-star angular separation. We used the
LIFEsim simulator to compute the integration time ($t_{int}$) required to
detect each planet with LIFE. A planet is considered detectable if a broadband
signal-to-noise ratio $S/N$=7 is achieved over the spectral range $4-18.5\mu$m
in $t_{int}\leq$100 hours. We tested whether the planet is accessible to HWO in
reflected starlight based on its notional inner and outer working angles, and
minimum planet-to-star contrast. LIFE's reference configuration (four 2-m
telescopes with 5% throughput and a nulling baseline between 10-100 m) can
detect 212 known planets within 20 pc. Of these, 55 are also accessible to HWO
in reflected starlight, offering a unique opportunity for synergies in
atmospheric characterization. LIFE can also detect 32 known transiting
exoplanets. Furthermore, 38 LIFE-detectable planets orbit in the habitable
zone, of which 13 with $M_p<5M_\oplus$ and 8 with $5M_\oplus<M_p<10M_\oplus$.
LIFE already has enough targets to perform ground-breaking analyses of
low-mass, habitable-zone exoplanets, a fraction of which will also be
accessible to other instruments.
