  As lower-mass stars often host multiple rocky planets, gravitational
interactions among planets can have significant effects on climate and
habitability over long timescales. Here we explore a specific case, Kepler-62f,
a potentially habitable planet in a five-planet system with a K2V host star.
N-body integrations reveal the stable range of initial eccentricities for
Kepler-62f is $0.00 \leqslant e \leqslant 0.32$, absent the effect of
additional, undetected planets. We simulate the tidal evolution of Kepler-62f
in this range and find that, for certain assumptions, the planet can be locked
in a synchronous rotation state. Simulations using LMD Generic GCM indicate
that with 3 bars of CO$_2$ in its atmosphere, Kepler-62f would only be warm
enough for surface liquid water at the upper limit of this eccentricity range,
providing it has a high planetary obliquity (between 60$^\circ$ and
90$^\circ$). A climate similar to modern-day Earth is possible for the entire
range of stable eccentricities if atmospheric CO$_2$ is increased to 5-bar
levels. In a low-CO$_2$ case, simulations with CCSM4 and LMD Generic GCM
indicate that increases in planetary obliquity and orbital eccentricity coupled
with an orbital configuration that places the summer solstice at or near
pericenter permit regions of the planet with above-freezing surface
temperatures. This may melt ice sheets formed during colder seasons. If
Kepler-62f is synchronously rotating and has an ocean, CO$_2$ levels above 3
bars would be required to distribute enough heat to the night side of the
planet to avoid atmospheric freeze-out and permit a large enough region of open
water at the planet's substellar point to remain stable. Overall, we find
multiple plausible combinations of orbital and atmospheric properties that
permit surface liquid water on Kepler-62f.
