We give a summary of radio molecular-line and infrared imaging observations of the newly found O-rich protoplanetary nebula, IRAS 19312+1950. This object exhibits a bipolar nebulosity of size ~ 30″ on the near-IR (JHK) images. A ring-like structure with a diameter of about 10″ is seen surrounding the central star. Toward this object, we detected thermal lines of CO, HCO+, SO, and SiO (O-bearing) molecules and CN, CS, HNC, NH3, N2H+, and HC3N (C- and N-bearing) molecules, as well as H2O and SiO masers lines. The line profiles of 12CO, HCN, SO, and HCO+ are composed of broad (Δv ~ 30–40 km s-1) and narrow (Δv < 5 km s-1) components. The SiO profile (J = 2—1 v = 0 thermal line) has only broad component, and the line profiles of non-O-bearing molecules (except HCN) have only a narrow component. Both components are spatially strongly peaked in intensity at the center of this object within a ~ 15″ telescope beam. We infer that both components originate from cool material surrounding the central star. This object is most likely an O-rich protoplanetary nebula with high mass loss rate and envelope chemistry similar to that of OH 231.8+0.4.