High-mass stars (with 8 Solar masses or larger) have strong impacts on various field of astrophysics and astrochemistry. However, their formation processes have been long-standing issues because of observational difficulties such as extremely large opacity of interstellar dust in high-mass star-forming regions except for centimeter to submillimeter wavelengths, larger distances and more complex structures in young high-mass clusters compared with low-mass star-forming regions, and smaller number of high-mass young stellar objects due to shorter evolutionary time scale. As a result, theoretical modeling is also challenging as basic properties of high-mass star-forming regions and newly born high-mass young stellar objects are still unclear. Very recent high resolution and high sensitivity observations with ALMA at millimeter/submillimeter wavelengths begin to overcome these observational difficulties. Number of infrared dark cloud cores and filaments, disks and outflows associated with high-mass young stellar objects have been observed at the highest resolution of 100-1000 au. These results provide initial condition, mass accretion and feedback processes, and chemical compositions in high-mass star-forming regions. I will review recent progress in high-mass star-formation studies in the ALMA era along with related observational and theoretical studies.