  The hundreds of multiple planetary systems discovered by the \textit{Kepler}
mission are typically observed to reside in close-in ($\lesssim0.5$ AU),
low-eccentricity, and low-inclination orbits. We run N-body experiments to
study the effect that unstable outer ($\gtrsim1$ AU) giant planets, whose end
orbital configurations resemble those in the Radial Velocity population, have
on these close-in multiple super-Earth systems. Our experiments show that the
giant planets greatly reduce the multiplicity of the inner super-Earths and the
surviving population can have large eccentricities ($e\gtrsim0.3$) and
inclinations ($i\gtrsim20^\circ$) at levels that anti-correlate with
multiplicity. Consequently, this model predicts the existence of a population
of dynamically hot single-transiting planets with typical eccentricities and
inclinations %in the ranges of $\sim 0.1-0.5$ and $\sim 10^\circ-40^\circ$. We
show that these results can explain the following observations: (i) the recent
eccentricity measurements of \textit{Kepler} super-Earths from transit
durations; (ii) the tentative observation that single-transiting systems have a
wider distribution of stellar obliquity angles compared to the
multiple-transiting systems; (iii) the architecture of some eccentric
super-Earths discovered by Radial Velocity surveys such as HD\,125612c. Future
observations from \textit{TESS} will reveal many more dynamically hot single
transiting planets, for which follow up Radial Velocity studies will be able to
test our models and see whether they have outer giant planets.
