The paper discusses the generation of primordial black holes (PBHs) and induced gravitational waves (GWs) through the enhancement of the power spectrum of primordial curvature perturbations, which is often accompanied by non-Gaussianity. The author reviews how non-Gaussianity arises in single-field inflation and the curvaton scenario, and then explains how to calculate the PBH mass function and induced GWs with such non-Gaussianities. When the PBH abundance is fixed, non-Gaussianity only slightly affects the spectral shape of the induced GWs, making it robust for mHz and nHz GW experiments. PBHs form when the density contrast exceeds a critical value, and their mass depends on the horizon mass at the re-entry moment. The abundance of PBHs depends on the number of Hubble patches that can satisfy the formation criterion. The Press-Schechter formalism, based on the compaction function, is used to calculate the PBH abundance, but it assumes Gaussian curvature perturbations. Non-Gaussianity can significantly alter the relation between the PBH abundance and the induced GW spectrum, as the induced GWs depend on the variance of the curvature perturbation PDF, while the PBH abundance depends on the high-$\sigma$ tail. The paper also discusses typical inflation models that can generate large non-Gaussianity, such as ultra-slow-roll inflation, constant-roll inflation with a bumpy potential, single-field inflation with a piecewise quadratic potential, and the curvaton scenario. These models can enhance the power spectrum of the curvature perturbation, leading to an increased PBH abundance and induced GW spectrum. The non-Gaussianity can be described by a perturbative series, and the $\delta N$ formalism is used to derive the fully nonlinear curvature perturbation. The paper concludes by discussing future topics, including the observational implications of non-Gaussianity in PBH formation and induced GW generation.The paper discusses the generation of primordial black holes (PBHs) and induced gravitational waves (GWs) through the enhancement of the power spectrum of primordial curvature perturbations, which is often accompanied by non-Gaussianity. The author reviews how non-Gaussianity arises in single-field inflation and the curvaton scenario, and then explains how to calculate the PBH mass function and induced GWs with such non-Gaussianities. When the PBH abundance is fixed, non-Gaussianity only slightly affects the spectral shape of the induced GWs, making it robust for mHz and nHz GW experiments. PBHs form when the density contrast exceeds a critical value, and their mass depends on the horizon mass at the re-entry moment. The abundance of PBHs depends on the number of Hubble patches that can satisfy the formation criterion. The Press-Schechter formalism, based on the compaction function, is used to calculate the PBH abundance, but it assumes Gaussian curvature perturbations. Non-Gaussianity can significantly alter the relation between the PBH abundance and the induced GW spectrum, as the induced GWs depend on the variance of the curvature perturbation PDF, while the PBH abundance depends on the high-$\sigma$ tail. The paper also discusses typical inflation models that can generate large non-Gaussianity, such as ultra-slow-roll inflation, constant-roll inflation with a bumpy potential, single-field inflation with a piecewise quadratic potential, and the curvaton scenario. These models can enhance the power spectrum of the curvature perturbation, leading to an increased PBH abundance and induced GW spectrum. The non-Gaussianity can be described by a perturbative series, and the $\delta N$ formalism is used to derive the fully nonlinear curvature perturbation. The paper concludes by discussing future topics, including the observational implications of non-Gaussianity in PBH formation and induced GW generation.