  Using a general circulation model (GCM), we investigate trends in simulated
hot Jupiter atmospheres for a range of irradiation temperatures (1,500 - 4,000
K), surface gravities (10 and 40 m s-2), and cloud conditions. Our models
include simplified temperature-dependent clouds with radiative feedback and
show how different cloud compositions, vertical thicknesses, and opacities
shape hot Jupiters atmospheres by potentially increasing planetary albedos,
decreasing photospheric pressures and nightside temperatures, and in some cases
producing strong dayside thermal inversions. With decreasing irradiation,
clouds progressively form on the nightside and cooler western limb followed by
the eastern limb and central dayside. We find that clouds significantly modify
the radiative transport and affect the observable properties of planets colder
than T_irr ~ 3,000~K (T_eq~2,100 K) depending on the clouds' vertical extent.
The precise strength of expected effects depends on the assumed parameters, but
trends in predicted phase curves emerge from an ensemble of simulations. Clouds
lead to larger phase curve amplitudes and smaller phase curve offsets at IR
wavelengths, compared to cloud-free models. At optical wavelengths, we predict
mostly westward phase curve offsets at intermediate temperatures (T_irr ~ 2,000
- 3,500 K) with clouds confined to the nightside and western limb. If clouds
are vertically compact (i.e. on order of a pressure scale height in thickness),
their distributions and effects become more complicated as different
condensates form at different heights -- some too deep to significantly affect
the observable atmosphere. Our results have implications for interpreting the
diversity of phase curve observations of planets with T_irr <~3,000~K.
