  We provide mass-loss rate predictions for O stars from Large and Small
Magellanic Clouds. We calculate global (unified, hydrodynamic) model
atmospheres of main sequence, giant, and supergiant stars for chemical
composition corresponding to Magellanic Clouds. The models solve radiative
transfer equation in comoving frame, kinetic equilibrium equations (also known
as NLTE equations), and hydrodynamical equations from (quasi-)hydrostatic
atmosphere to expanding stellar wind. The models allow us to predict wind
density, velocity, and temperature (consequently also the terminal wind
velocity and the mass-loss rate) just from basic global stellar parameters. As
a result of their lower metallicity, the line radiative driving is weaker
leading to lower wind mass-loss rates with respect to the Galactic stars. We
provide a formula that fits the mass-loss rate predicted by our models as a
function of stellar luminosity and metallicity. On average, the mass-loss rate
scales with metallicity as $ \dot M\sim Z^{0.59}$. The predicted mass-loss
rates are lower than mass-loss rates derived from H$\alpha$ diagnostics and can
be reconciled with observational results assuming clumping factor
$C_\text{c}=9$. On the other hand, the predicted mass-loss rates either agree
or are slightly higher than the mass-loss rates derived from ultraviolet wind
line profiles. The calculated \ion{P}{v} ionization fractions also agree with
values derived from observations for LMC stars with
$T_\text{eff}\leq40\,000\,$K. Taken together, our theoretical predictions
provide reasonable models with consistent mass-loss rate determination, which
can be used for quantitative study of stars from Magellanic Clouds.
