Andrei Linde discusses two hybrid inflation models in this paper. The first model describes inflation ending through a rapid rolling (waterfall) of a scalar field $\sigma$ triggered by another scalar field $\phi$. This model combines chaotic inflation with a potential $V(\phi) = \frac{m^2 \phi^2}{2}$ and spontaneous symmetry breaking with a potential $V(\sigma) = \frac{1}{4 \pi} (M^2 - \lambda \sigma^2)^2$. The last stages of inflation are supported by the 'non-inflationary' potential $V(\sigma)$. The second model is a hybrid of extended inflation (Brans-Dicke theory), new inflation (phase transition due to a non-minimal coupling of the inflaton field to gravity), and chaotic inflation. In this model, inflation ends through a slow rolling of the field $\phi$, avoiding the big-bubble problem of extended inflation. The model has a second-order phase transition and does not suffer from the same issues as the extended inflation scenario. Linde also discusses the possibility of different domains in the universe with varying Planck masses and density perturbation amplitudes, which can be realized through the self-reproduction of the universe in the context of these hybrid models. These models offer a rich variety of inflationary theories with interesting and sometimes unusual properties, enhancing the possibility of finding a correct description of observational data within inflationary cosmology.Andrei Linde discusses two hybrid inflation models in this paper. The first model describes inflation ending through a rapid rolling (waterfall) of a scalar field $\sigma$ triggered by another scalar field $\phi$. This model combines chaotic inflation with a potential $V(\phi) = \frac{m^2 \phi^2}{2}$ and spontaneous symmetry breaking with a potential $V(\sigma) = \frac{1}{4 \pi} (M^2 - \lambda \sigma^2)^2$. The last stages of inflation are supported by the 'non-inflationary' potential $V(\sigma)$. The second model is a hybrid of extended inflation (Brans-Dicke theory), new inflation (phase transition due to a non-minimal coupling of the inflaton field to gravity), and chaotic inflation. In this model, inflation ends through a slow rolling of the field $\phi$, avoiding the big-bubble problem of extended inflation. The model has a second-order phase transition and does not suffer from the same issues as the extended inflation scenario. Linde also discusses the possibility of different domains in the universe with varying Planck masses and density perturbation amplitudes, which can be realized through the self-reproduction of the universe in the context of these hybrid models. These models offer a rich variety of inflationary theories with interesting and sometimes unusual properties, enhancing the possibility of finding a correct description of observational data within inflationary cosmology.